Over the past decade, tremendous progress has been made in understanding the structural properties of our galaxy. A combination of data from large-scale photometric, spectroscopic, and astrometric stellar surveys, such as the Gaia-ESO, LAMOST, GALAH, APOGEE allowed robust constraints on the temporal variability of chemical enrichment across the Galactic disc, bulge, and the halo [1]}, [2]}, [3]}. Complemented with accurate positions and kinematics of stars from the Gaia space mission [4]}, [5]}, [6]}, it has become possible to constrain the detailed chemo-dynamical evolution of these stellar populations and to gain new insights into their origins.
